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\@writefile{toc}{\contentsline {section}{\numberline {A}Project Description}{1}}
\@writefile{toc}{\contentsline {subsection}{\numberline {A. 1}Results from Prior NSF Support}{1}}
\@writefile{toc}{\contentsline {subsection}{\numberline {A. 2}Overview of the Project}{1}}
\@writefile{lof}{\contentsline {figure}{\numberline {1}{\ignorespaces  \relax \fontsize  {10}{12}\selectfont  \abovedisplayskip 10\p@ plus2\p@ minus5\p@ \abovedisplayshortskip \z@ plus3\p@ \belowdisplayshortskip 6\p@ plus3\p@ minus3\p@ \def \leftmargin \leftmargini \parsep 4.5\p@ plus2\p@ minus\p@ \topsep 9\p@ plus3\p@ minus5\p@ \itemsep 4.5\p@ plus2\p@ minus\p@ {\leftmargin \leftmargini \topsep 6\p@ plus2\p@ minus2\p@ \parsep 3\p@ plus2\p@ minus\p@ \itemsep \parsep }\belowdisplayskip \abovedisplayskip Schematic of the 1.6 m off-axis, open NST for which the primary mirror is as close to the declination axis as possible. The optical path is indicated. There is a Nasmyth-focus along the declination axis, where we can put instrumentation. In this design, the coud\'e mirror is simply a flip mirror to re-direct light from the declination axis to the floor below, where the AO and principal instrumentation reside.}}{2}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {A. 2.1}NJIT Support for BBSO Programs}{3}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {A. 2.2}Heritage and Goals of the NST}{3}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {A. 2.3}NST, BBSO and Other Solar Observatories}{4}}
\@writefile{toc}{\contentsline {subsection}{\numberline {A. 3}Science Drivers for the NST}{5}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {A. 3.1}High Resolution, High Cadence Studies of Solar Flares}{5}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {A. 3.2}Structure and Evolution of Magnetic Fields in Flaring Active Regions}{6}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {A. 3.3}Dynamics of Kilogauss Flux Tubes}{6}}
\@writefile{lof}{\contentsline {figure}{\numberline {2}{\ignorespaces \relax \fontsize  {10}{12}\selectfont  \abovedisplayskip 10\p@ plus2\p@ minus5\p@ \abovedisplayshortskip \z@ plus3\p@ \belowdisplayshortskip 6\p@ plus3\p@ minus3\p@ \def \leftmargin \leftmargini \parsep 4.5\p@ plus2\p@ minus\p@ \topsep 9\p@ plus3\p@ minus5\p@ \itemsep 4.5\p@ plus2\p@ minus\p@ {\leftmargin \leftmargini \topsep 6\p@ plus2\p@ minus2\p@ \parsep 3\p@ plus2\p@ minus\p@ \itemsep \parsep }\belowdisplayskip \abovedisplayskip (Left) Schematic of the new open telescope and its retractable dome (not to scale). Typically, the light goes to the Fabry-P\'erot-based scientific channels in the visible and near-IR, labelled FP(V) and FP(IR), which reside on the horizontal optical tables. The optical tables are installed on the floor beneath the telescope. Future Far-IR (FIR) instrumentation would require only a tip/tilt mirror (TTM) to get diffraction-limited images. The visible and near-IR channels would be operating downstream of the high-order AO system. We anticipate placing the polarizing optics between M2 and M3, where the light is nearly parallel. (Right) The optical layout of the NST with a true relative scale (a Zemax created model). The NST is an off-axis section of a conventional Gregory telescope with parabolic primary mirror M1, elliptical secondary M2, removable (for access to the primary focal plane with a wide FOV) heat-stop mirror HS, flat folding mirrors M3 and M4 (coud\'e mirror). M3 is a fixed folding mirror. The off-axis primary has an f-ratio 2.4 (parent's f-ratio is about 0.73). The telescope's effective focal length is about 80 m with a final f-ratio of 50, which is close to that of the current 65\nobreakspace  {}cm telescope. The image scale in the Gregory-Coud\'e focal plane is 2.6$''$/mm. TTM redirects light to the floor below to get diffraction-limited images for far-IR instrumentation.}}{7}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {A. 3.4}Heating of the Upper Atmosphere}{7}}
\@writefile{toc}{\contentsline {subsection}{\numberline {A. 4}The 1.6\nobreakspace  {}m NST}{8}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {A. 4.1}Technical Overview}{8}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {A. 4.2}Telescope Optics}{9}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {A. 4.3}Mechanical Structure}{10}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {A. 4.4}Control Systems}{10}}
\@writefile{toc}{\contentsline {subsection}{\numberline {A. 5}Adaptive Optics}{10}}
\@writefile{toc}{\contentsline {subsection}{\numberline {A. 6}New Scientific Instrumentation for the NST}{11}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {A. 6.1}Visible Light Vector Magnetographs}{11}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {A. 6.2}Infrared Vector Magnetograph}{12}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {A. 6.3}Real--Time Image Reconstruction (RTIR)}{12}}
\@writefile{toc}{\contentsline {subsection}{\numberline {A. 7}Project Organization and Management}{13}}
\@writefile{lof}{\contentsline {figure}{\numberline {3}{\ignorespaces \relax \fontsize  {10}{12}\selectfont  \abovedisplayskip 10\p@ plus2\p@ minus5\p@ \abovedisplayshortskip \z@ plus3\p@ \belowdisplayshortskip 6\p@ plus3\p@ minus3\p@ \def \leftmargin \leftmargini \parsep 4.5\p@ plus2\p@ minus\p@ \topsep 9\p@ plus3\p@ minus5\p@ \itemsep 4.5\p@ plus2\p@ minus\p@ {\leftmargin \leftmargini \topsep 6\p@ plus2\p@ minus2\p@ \parsep 3\p@ plus2\p@ minus\p@ \itemsep \parsep }\belowdisplayskip \abovedisplayskip This Gantt chart summarizes the NST development and implementation timelines. The parts of the NST that would be funded by the MRI are shown solid blue and the parts that would {\it  not} be supported by the MRI are shown in red with vertical lines. The critical time path for the NST is determined by the fabrication of the primary blank (including skeletal mirror cell) and the design of the optical support structure. These relatively inexpensive parts of the project need to be started before MRI funding to ensure first light in late 2005. The critical and expensive parts of the project are proposed for here, and include building and implementing the mirror cell, the optical support structure the thermal control and computer control systems. The instrument complement for the NST will be on-line in mid-2004 (separate funding) and the retractable dome (separate funding) will be installed along with the NST. }}{14}}
\@writefile{toc}{\contentsline {section}{\numberline {B}References}{16}}
\@writefile{toc}{\contentsline {section}{\numberline {C}Budget}{17}}